# Solar energetic particle propagation in wave turbulence and the possibility of wave generation

## TL;DR

This paper models the propagation of solar energetic electrons in turbulent magnetic fields, incorporating dynamical effects and wave growth, to better understand particle transport and turbulence interactions near the Sun.

## Contribution

It introduces a physics-first simulation approach with dynamical perpendicular diffusion and wave growth effects, advancing the understanding of particle-turbulence interactions.

## Key findings

- Reasonable qualitative agreement with observations
- Wave growth significantly alters turbulence levels near the Sun
- Inclusion of dynamical effects improves propagation modeling

## Abstract

A complete theory for the complex interaction between solar energetic particles and the turbulent interplanetary magnetic field remains elusive. In this work we aim to contribute towards such a theory by modelling the propagation of solar energetic particle electrons in plasma wave turbulence. We specify a background turbulence spectrum, as constrained through observations, calculate the transport coefficients from first principles, and simulate the propagation of these electrons in the inner heliosphere. We have also, for the first time, included dynamical effects into the perpendicular diffusion coefficient. We show that such a "physics-first" approach can lead to reasonable results, when compared qualitatively to observations. In addition, we include the effect of wave growth/damping due to streaming electrons and show that these particles can significantly alter the turbulence levels close to the Sun for the largest events.